Rayleigh–Taylor instability in magnetohydrodynamic simulations of the Crab nebula
Rayleigh–Taylor instability in magnetohydrodynamic simulations of the Crab nebula
复制标题
蟹状星云磁流体动力学模拟中的瑞利-泰勒不稳定性
DOI：
10.1093/mnras/stu1082
复制
发表时间：
2014
影响因子：
4.8
通讯作者：
R. Keppens
中科院分区：
文献类型：
--
作者：
O. Porth;S. Komissarov;R. Keppens
在本文中，我们讨论了脉冲星风星云（PWN）轴对称模拟中瑞利-泰勒（RT）细丝的发展。高分辨率自适应网格细化磁流体动力学模拟用于解决不稳定性的非线性演化。细丝的典型分离是由星云中的湍流和细丝的分层生长介导的。最近的 PWN 全球三维模拟中发现的强磁耗散和场随机化表明，磁张力不足以抑制 RT 细丝的生长，这与蟹状星云中突出细丝的观测结果一致。这里提出的长期轴对称结果证实了这一发现。
In this paper, we discuss the development of Rayleigh-Taylor (RT) filaments in axisymmetric simulations of pulsar wind nebulae (PWN). High-resolution adaptive mesh refinement magnetohydrodynamic simulations are used to resolve the non-linear evolution of the instability. The typical separation of filaments is mediated by the turbulent flow in the nebula and hierarchical growth of the filaments. The strong magnetic dissipation and field randomization found in recent global three-dimensional simulations of PWN suggest that magnetic tension is not strong enough to suppress the growth of RT filaments, in agreement with the observations of prominent filaments in the Crab nebula. The long-term axisymmetric results presented here confirm this finding.